arXiv2001
We examine the status of various dark energy-models in light of the recently observed SN 1997ff at z \approx 1.7. The modified data still fit a pure cosmological constant Λor a quintessence with an equation of state similar to that of Λ. The kinematical Λ-models, Λ\sim S^{-2} and Λ\sim H^2, also fit the data reasonably well and require less dark energy density than is required by the constant Λ-model. However, the model Λ\sim S^{-2} with low energy density becomes unphysical as it cannot accommodate higher redshift objects. We also examine an alternative explanation of the data, viz., the absorption by the intervening whisker-like dust and find that the quasi-steady state model and the FRW model Ω_{\rm m0}=0.33, {\it without any dark energy} also fit the data reasonably well. We notice that the addition of SN 1997ff to the old data has worsened the fit to most of the models, except a closed FRW model with a constant Λand a closed quintessence-model with ω_ϕ=-0.82, and the models have started departing from each other as we go above z=1. However, to make a clear discrimination possible, a few more supernovae with z>1 are required. We have also calculated the age of the universe in these models and find that, in the models with a constant Λ, the expansion age is uncomfortably close to the age of the globular clusters. Quintessence-models show even lower age. The kinematical Λ-models are, however, interesting in this connection (especially the model Λ\sim H^2), which give remarkably large age of the universe.